| Related sites for http://cfa-www.harvard.edu/afoe/espd.html |
| List_of_links_treating_of_extrasolar_planets_and_their_detection This page presents a list of carefully selected links to very informative sites about extra solar planets. | | Microlensing_Observations_in_Astrophysics_(MOA) A joint Japanese/New Zealand project established to carry out astrophysical observations using a gravitational microlensing technique. Applications include research for extra-solar planets, dark matt | | Microvariability_and_Oscillations_os_STars Detection and characterisation of: (1) acoustic oscillations in Sun-like stars, including very old stars (metal-poor subdwarfs) and magnetic stars (roAp), to probe seismically their structures and age | | Mid-InfraRed_Large-well_Imager MIRLIN - The JPL Deep-Well Mid-Infrared Array Camera | | Nova_Celestia_-_A_Guide_to_Extrasolar_Planets Contains information and free illustrations of Extrasolar planets (carbon planets, gas giants and terrestrial planets), detection methods and missions. | | The_Optical_Gravitational_Lensing_Experiment_(OGLE) A long term project with the main goal of searching for the dark matter with microlensing phenomena. | | Optical_Long_Baseline_Interferometry_News NASA JPL's Optical Long Baseline Interferometer project homepage. 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Extrasolar Planet Detection with the AFOE Extrasolar Planet Detection with the AFOE  Detection of a high-eccentricity low-mass companion to HD 89744IntroductionExtrasolar planet detection is the search for planets around other stars thanour Sun. Several techniques are being used to detect planets around othersuns; they are discussed in a Scientific American Exploration Web page. The AFOE has been designed to provide therequired precison and stability to detect the wobble induced on the star bythe presence of a planet.Indeed, both the planet and the star revolve around their commoncenter of gravity. While the center of gravity is very close to the center ofthe star, it is not exactly at the center of the star.Therefore the star wobbles around the center of gravity with the sameperiod as the planet. The more massive the planet and the closer the orbit thelarger will be the amplitude of the wobble.By measuring the doppler shift caused by thewobble of the star on the light it emits, we can detect such a periodicmotion.This wobble is very small, therefore very stable and precise measurements areneeded to make such a detection. The amplitude if the wobble induced byJupiter on the Sun is 13 meters per second, or 29 miles per hour (1 m/s is2.237 mph).Animations for some simulations of orbit are nowavailable.ResultsThe AFOE has developed a planet detectionprogram since 1992. As of 1995, the instrument configuration became stableenough to achieve the required precision.The AFOE extrasolar program has since detected a high-eccentricity low-mass companion to HD 89744. detected a multiple planetary system around the star Upsilon Andromedae. detected a planet around the star rho Coronae Borealis. confirmed the presence of a 3.9 Jupiter mass planet around the star tau Boötis. confirmed the presence of a 0.5 Jupiter mass planet around the star 51 Pegasi. Presented at the 194th AAS meeting: "Evidence for a System of planets orbiting upsilon Andromedae", a poster presentation showing the evidence for a system of 3 giant planets around the star Upsilon Andromedae and the results of dynamical stability calculations to further contrain the properties of the system. Published in The Astrophysical Journal Letter (v. 494, p. L85) "A Search for Line Shape and Depth Variations in 51 Pegasi and Tau Boötis" , where our analysis of spectroscopic observations of 51 Pegasi and tau Boötis with the AFOE show no periodic changes in the shapes of their line profiles; these results for 51 Peg are in significant conflict with those reported by Gray and Hatzes (1997). Published in The Astrophysical Journal Supplement (v. 117, p. 563-85) "Exoplanets or Dynamic Atmospheres? The Radial Velocity and Line Shape Variations of 51Pegasi and Tau Boötis. " , where we present expanded and detailed analysis of spectroscopic observations of 51 Pegasi and tau Boötis, that show no evidence for periodic line-shape changes,at a level that rules out pulsations as the source of the radial velocity variability. Presented a talk at IAU Colloquium 170 on Precise Stellar Radial Velocities , Victoria, BC, June 1998: The advanced fiber-optic echelle (AFOE) and extrasolar planet searches, where we discuss the status of the instrument, as well as an upgrade to the instrument, a Fabry-Perot reference, which may prove important both for the AFOE and for all Precision Radial Velocity (PRV) facilities. Presented a poster at IAU Colloquium 170 on Precise Stellar Radial Velocities , Victoria, BC, June 1998: "The Planet Orbiting RhoCrB" , where we present updated orbital parameters of rhoCrB, and discuss various planet formation scenarios in view of the observational constrains. Presented a poster at The 10th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun , Cambridge, July 1997: "51 Pegasi and Tau Boötis: Planets or Pulsations", where we discuss the suggestion (Gray 1997) that the radial velocity variations observed in the spectra of 51 Pegasi are the result of stellar pulsations as opposed to the reflex motion due to an orbital companion. References ExoplanetResearch with the Advanced Fiber Optic Echelle, Korzennik etal., 1997, poster presented at the 10th Cool Star Meeting (July 1997,Cambridge, MA The AFOE Program for Extra Solar PlanetResearch, Noyes et al., 1997, in "Planets Beyond the SolarSystem and the Next Generation of Space Missions", Space Telescope ScienceInstitute Workshop, P.A.S.P., in press. HD 3346., Noyes, R., Korzennik, S., Nisenson, P., Jha, S.,Krockenberger, M., Brown, T., Kennelly, T., Rowland, C., Horner, S., 1996,IAUCirc. 6316. Precise Radial Velocity Measurements of 51 Pegasi with the AFOESpectrograph Kennelly, E.J., Brown, T. M., Rowland, C., Horner, S.D.,Korzennik, S.G., Krockenberger, M., Nisenson, P., Noyes, R.W., 1995, BAAS,187, 7005.Other Sites Tim Brown's STellar Astrophysics & Research on Exoplanets project (aka STARE) Web page. STARE uses precise time-series photometry to search for extrasolar giant planets transiting their parent stars. Jean Schneider's Extrasolar Planets Encyclopaedia (France), or the US mirror site. The San Francisco State University Planet Search Project Web page.This celestial map shows where to find 11of the stars known to have planetary companions (and growing...).A compressed PostScript version of themap is also available.  AFOE Home page.__________________________________________________Sylvain G. Korzennik (skorzennik@cfa.harvard.edu)Adam Contos (acontos@cfa.harvard.edu)Last modified: Thu Jan 30 10:18:39 2003 |
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